UBVJHKLM photometry of the symbiotic Mira V407 Cyg in 1998–2002

Kolotilov, E. A.; Шенаврин, В. И.; Shugarov, S. Yu.; Yudin, B. F.

doi:10.1134/1.1611218

Cited by 27 publications

(37 citation statements)

References 14 publications

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“…On these occasions, the optical emission of the WD rivaled that of the Mira star at its maximum and then slowly declined over the following several years. These flares are typical of all symbiotic binaries and probably result from changes in the accretion rate (Kolotilov et al 2003). In 2010, V407 Cyg was observed on March 10.813 (UT) at V = 7, about 5 mag above the maximum of the Mira cycle, a brightness level never reached before in the photometric history of the system (Nishiyama et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Particle acceleration and non-thermal emission during the V407 Cygni nova outburst

Martin

Dubus

2013

A&A

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Context. On March 2010, the symbiotic binary V407 Cyg erupted as a result of a nova explosion. The event gave rise to a two-week long burst of ≥100 MeV γ-rays detected by Fermi/LAT, a unique observation testifying to particle acceleration in the system. Aims. The outburst can be considered a scaled-down supernova, with short dynamical time scale, and thus can constitute a test case for theories of the origin of Galactic cosmic rays. We aim at determining the properties of the accelerated particles and identifying the origin of the high-energy radiation. Methods. We developed a model for diffusive shock acceleration and non-thermal emission in V407 Cyg, complemented by an evaluation of the thermal emission from the shocked plasma. We considered both leptonic and hadronic contributions to the non-thermal processes, and investigated the effect of many binary and nova parameters.Results. The γ-ray emission is mostly of leptonic origin and arises predominantly from inverse-Compton scattering of the nova light. Matching the light curve requires gas accumulation in the vicinity of the white dwarf, as a consequence of wind accretion, while the spectrum imposes particle scattering close to the Bohm limit in the upstream equipartition magnetic field. The nova accelerated protons (respectively electrons) with energies up to 300 GeV (respectively 20 GeV), for a total non-thermal energy 10 43 erg after two weeks, representing 10% of the initial nova kinetic energy. The electron-to-proton ratio at injection is 6%. Conclusions. The V407 Cyg eruption can be understood from the same principles that are invoked for particle acceleration in supernova remnants, although without the need for strong magnetic field amplification. The population of novae in symbiotic systems is a negligible source of Galactic cosmic rays, and most likely not a class of TeV-emitters.

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Section: Introductionmentioning

confidence: 99%

Particle acceleration and non-thermal emission during the V407 Cygni nova outburst

Martin

Dubus

2013

A&A

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“…Since that time, it has been observed to periodically increase in brightness according to the long-period Mira, and minor, slowly developing outbursts, never becoming brighter than approximately V = 11.5 during the years 1984-1995(Kolotilov et al 1998. A slowdeveloping outburst in the late 1990s was identified from the light curve (Kolotilov et al 2003;Shugarov et al 2007), as it was claimed to become brighter than the outburst of 1936, but never being brighter than V ∼ 11.8. Large gaps in the light curve exist from the discovery data epoch until around 1990, which are of sufficient duration to have missed any outburst similar to the current event.…”

Section: Introductionmentioning

confidence: 99%

The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst

Shore

Wahlgren

Augusteijn

et al. 2011

A&A

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Context. V407 Cyg was, before 2010 Mar., known only as a D-type symbiotic binary system in which the Mira variable has a pulsation period of approximately 750 days, one of the longest known. On 2010 Mar. 10, it was discovered in outburst, eventually reaching V < 8. This is the first recorded nova event for this system, but it closely resembles the spectroscopic development of RS Oph, the prototypical symbiotic-like recurrent nova. It was also detected by Fermi above 100 MeV and displayed strong, likely nonthermal centimeter wavelength radio emission. Aims. Unlike classical novae occurring in compact cataclysmic binary systems, for which the ejecta undergo free ballistic expansion, this explosion occurred within the dense, complex wind of a Mira variable companion. This paper concentrates on the development of the shock and its passage through the Mira wind. We also present some constraints on the binary system properties. Methods. Using medium and high resolution ground-based optical spectra, visual and Swift UV photometry, and Swift X-ray spectrophotometry, we describe the behavior of the high-velocity profile evolution for this nova during its first three months. Results. Using the diffuse interstellar bands visible in the high-resolution optical spectra, we obtain an extinction E(B − V) ≈ 0.45 ± 0.05. The spectral type of the red giant during this period, when the star was at R minimum, was no earlier than M7 III. The peak of the X-ray emission occurred at about day 40 with a broad maximum and decline after day 50. The main changes in the optical spectrum began at around that time. The He II 4686 Å line first appeared between days 7 and 14 and initially displayed a broad, symmetric profile that is characteristic of all species before day 60. The profile development thereafter depended on ionization state. Low-excitation lines remained comparatively narrow, with v rad,max of order 200-400 km s −1 . They were systematically more symmetric than lines such as [Ca V], [Fe VII], [Fe X], and He II, all of which showed a sequence of profile changes going from symmetric to a blue wing similar to that of the low ionization species but with a red wing extended to as high as 600 km s −1 . The [O I] 6300, 6364 doublet showed a narrow wind-emission component near the rest velocity of the system and a broad component, 200-300 km s −1 , whose relative intensity increased in time. Forbidden lines of N II and O III had two separate contributors to the profiles, a broad line that increased in strength and velocity width, exceeding 200 km s −1 , and narrow components from a surrounding ionized region at higher velocity than the Mira wind. The Na I D doublet developed a broad component with similar velocity width to the other low-ionization species. The O VI Raman features observed in recent outbursts of RS Oph were not detected. We interpret these variations as aspherical expansion of the ejecta within the Mira wind. The blue side is from the shock penetrating into the wind while the red wing is from the low-density peri...

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“…Flickering on a timescale of several tens of minutes with an amplitude of 0.2 mag was detected in the V band (Kolotilov et al 2003). Such variability is usually related to existence of an accretion disk in the system.…”

Section: Observationsmentioning

confidence: 97%

“…1. The dates of Mira maxima in the B band were calculated using the ephemeris from Kolotilov et al (2003):…”

Section: Observationsmentioning

confidence: 99%

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Four states of the recurrent symbiotic nova V407 Cyg

et al. 2013

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UBVJHKLM photometry of the symbiotic Mira V407 Cyg in 1998–2002

Cited by 27 publications

References 14 publications

Particle acceleration and non-thermal emission during the V407 Cygni nova outburst

Particle acceleration and non-thermal emission during the V407 Cygni nova outburst

The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst

Four states of the recurrent symbiotic nova V407 Cyg

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